Authors: Valeri P Frolov
Publish Date: 2014/05/12
Volume: 2014, Issue: 5, Pages: 49-
Abstract
In a classical description the spacetime curvature inside a black hole infinitely grows In the domain where it reaches the Planckian value and exceeds it the Einstein equations should be modified In the absence of reliable theory of quantum gravity it is instructive to consider simplified models We assume that a spacetime curvature is limited by some value of the order of the Planckian one We use modified Vaidya metric proposed by Hayward to describe the black hole evaporation process In such a spacetime the curvature near r = 0 remains finite it does not have an event horizon and its apparent horizon is closed If the initial mass of such a ‘black hole’ is much larger than the Planckian one its properties as seen by an external observer are practically the same as properties of the ‘standard’ black hole with the event horizon We study outgoing null rays in the vicinity of the outer apparent horizon and introduce a notion of a quasihorizon We demonstrate that particles trapped inside a ‘black hole’ during the evaporation process finally may return to external space after the evaporation is completed We also demonstrate that such quanta would have very large blueshift The absence of the event horizon makes it possible restoration of the unitarity in evaporating black holesThis article is published under an open access license Please check the Copyright Information section for details of this license and what reuse is permitted If your intended use exceeds what is permitted by the license or if you are unable to locate the licence and reuse information please contact the Rights and Permissions team
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